J/A+A/640/A70 Massive discs in cosmological simulations (Marasco+, 2020)
Massive disc galaxies too dominated by dark matter in cosmological
hydrodynamical simulations.
Marasco A., Posti L., Oman K., Famaey B., Cresci G., Fraternali F.
<Astron. Astrophys. 640, A70 (2020)>
=2020A&A...640A..70M 2020A&A...640A..70M (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Galaxy catalogs
Keywords: galaxies: kinematics and dynamics - galaxies: halos -
galaxies: spiral - methods: numerical
Abstract:
We investigate the disc-halo connection in massive
(M*>5x1010M☉) disc galaxies from the cosmological
hydrodynamical simulations EAGLE and IllustrisTNG, and compare it with
that inferred from the study of HI rotation curves in nearby massive
spirals from the Spitzer Photometry and Accurate Rotation Curves
(SPARC) dataset. We find that discrepancies between the simulated and
observed discs arise both on global and on local scales. Globally, the
simulated discs inhabit halos that are a factor 4 (in EAGLE) and 2 (in
IllustrisTNG) more massive than those derived from the rotation curve
analysis of the observed dataset. We also use synthetic rotation
curves of the simulated discs to demonstrate that the recovery of the
halo masses from rotation curves are not systematically biased. We
find that the simulations predict dark-matter dominated systems with
stellar-to-total enclosed mass ratios that are a factor of 1.5-2
smaller than real galaxies at all radii. This is an alternative
manifestation of the `failed feedback problem', since it indicates
that simulated halos hosting massive discs have been too inefficient
at converting their baryons into stars, possibly due to an overly
efficient stellar and/or AGN feedback implementation.
Description:
We build our simulated galaxy sample using two suites of
very well-known, publicly available cosmological hydrodynamical
simulations of galaxy formation in the {LAMBDA}CDM framework: EAGLE
and IllustrisTNG. Both simulation suites follow selfconsistently the
formation and evolution of galaxies and of their environments, and
include treatments for star formation, stellar evolution, black-hole
accretion, feedback from supernovae and AGN, primordial and metal-line
gas cooling and, in the case of IllustrisTNG, the amplification and
evolution of seed magnetic fields. The parameters of both models are
calibrated to output a 'realistic' population of galaxies at z=0
in terms of their number densities, sizes, central black-hole masses
and star formation rates.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1e.dat 43 46 Data for simulated discs in EAGLE (Ref-L0100N1504)
tablea1t.dat 41 130 Data for simulated discs in IllustrisTNG (TNG100-1)
tablea2.dat 71 21 Data for nearby spirals from the SPARC sample
from Lelli et al., 2016, Cat. J/AJ/152/157
and Posti et al. (2019A&A...626A..56P 2019A&A...626A..56P)
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See also:
J/AJ/152/157 : Mass models for 175 disk galaxies with SPARC (Lelli+, 2016)
Byte-by-byte Description of file: tablea1e.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- ID Galaxy ID from the catalogue of McAlpine et al.,
2016, Astronomy and Computing, 15, 72
10- 14 F5.2 [Msun] logMs log10 of stellar mass (1)
16- 20 F5.2 [Msun] logMh log10 of halo mass
22- 27 F6.2 km/s vflat Circular speed at which the rotation curve
flattens
29- 33 F5.2 kpc Reff Half-mass radius
35- 38 F4.2 --- Rs Ratio between the median azimuthal speed
and the vertical velocity dispersion for
the stellar component
40- 43 F4.2 --- Fs Fraction of non counter-rotating stars (1)
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Note (1): Computed within a spherical radius of 30kpc.
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Byte-by-byte Description of file: tablea1t.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- ID Galaxy ID from the catalogue of Nelson et al.,
2019, Astronomy and Computing, 6, 2
8- 12 F5.2 [Msun] logMs log10 of stellar mass (1)
14- 18 F5.2 [Msun] logMh log10 of halo mass
20- 25 F6.2 km/s vflat Circular speed at which the rotation curve
flattens
27- 31 F5.2 kpc Reff Half-mass radius
33- 36 F4.2 --- Rs Ratio between the median azimuthal speed
and the vertical velocity dispersion for
the stellar component
38- 41 F4.2 --- Fs Fraction of non counter-rotating stars (1)
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Note (1): Computed within a spherical radius of 30kpc.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Galaxy Galaxy name
13- 17 F5.2 [Msun] logMs50 log10 of stellar mass, 50th percentile of
the posterior prob. distribution
19- 23 F5.2 [Msun] logMs16 16th percentile of the posterior
25- 29 F5.2 [Msun] logMs84 84th percentile of the posterior
31- 35 F5.2 [Msun] logMh50 log10 of halo mass, 50th percentile of the
posterior prob. distribution
37- 41 F5.2 [Msun] logMh16 16th percentile of the posterior
43- 47 F5.2 [Msun] logMh84 84th percentile of the posterior
49- 54 F6.2 km/s vflat HI rotational velocity taken at the flat
part of the rotation curve (1)
56- 60 F5.2 km/s e_vflat Uncertainty on vflat
62- 66 F5.2 kpc Reff Effective radius (from 3.6um SPITZER data)
68- 71 F4.2 kpc e_Reff Uncertainty on Reff
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Note (1): A value of 0 indicates that the rot.curve does not flatten.
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Acknowledgements:
Antonino Marasco, antonino.marasco(at)inaf.it
(End) Antonino Marasco [INAF-Arcetri, Italy], Patricia Vannier [CDS] 24-Jun-2020